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A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg² of SPTpol Temperature and Polarization Data

Wu, W. L. K. and Moran, C. Corbett and Crites, A. T. and Padin, S. (2019) A Measurement of the Cosmic Microwave Background Lensing Potential and Power Spectrum from 500 deg² of SPTpol Temperature and Polarization Data. Astrophysical Journal, 884 (1). Art. No. 70. ISSN 1538-4357. doi:10.3847/1538-4357/ab4186.

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We present a measurement of the cosmic microwave background lensing potential using 500 deg² of 150 GHz data from the SPTpol receiver on the South Pole Telescope. The lensing potential is reconstructed with signal-to-noise per mode greater than unity at lensing multipoles L ≾ 250, using a quadratic estimator on a combination of cosmic microwave background temperature and polarization maps. We report measurements of the lensing potential power spectrum in the multipole range of 100 < L < 2000 from sets of temperature-only (T), polarization-only (POL), and minimum-variance (MV) estimators. We measure the lensing amplitude by taking the ratio of the measured spectrum to the expected spectrum from the best-fit Λ cold dark matter model to the Planck 2015 TT + low P + lensing data set. For the minimum-variance estimator, we find A_(MV) = 0.944±0.058(Stat.)±0.025(Sys.) restricting to only polarization data, we find A_(POL) = 0.906±0.090(Stat.)±0.040(Sys.). Considering statistical uncertainties alone, this is the most precise polarization-only lensing amplitude constraint to date (10.1σ) and is more precise than our temperature-only constraint. We perform null tests and consistency checks and find no evidence for significant contamination.

Item Type:Article
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URLURL TypeDescription Paper
Wu, W. L. K.0000-0001-5411-6920
Moran, C. Corbett0000-0003-2088-7465
Additional Information:© 2019 The American Astronomical Society. Received 2019 May 14; revised 2019 July 31; accepted 2019 September 3; published 2019 October 14. The authors would like to acknowledge helpful comments from Chang Feng and Srinivasan Raghunathan on the manuscript. The South Pole Telescope program is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through grant GBMF No. 947 to the University of Chicago. This work is also supported by the U.S. Department of Energy. W.L.K.W. is supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. J.W.H. is supported by the National Science Foundation under award No. AST-1402161. C.R. acknowledges support from an Australian Research Council Future Fellowship (FT150100074). B.B. is supported by the Fermi Research Alliance LLC under contract No. De-AC02-07CH11359 with the U.S. Department of Energy. The Cardiff authors acknowledge support from the UK Science and Technologies Facilities Council (STFC). The CU Boulder group acknowledges support from NSF AST-0956135. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and the Fonds de Recherche du Québec—Nature et technologies. The UCLA authors acknowledge support from NSF AST-1716965 and CSSI-1835865. Work at Argonne National Lab is supported by UChicago Argonne LLC, Operator of Argonne National Laboratory (Argonne). Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated under contract No. DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under contract No. DE-AC02-05CH11231. The data analysis pipeline also uses the scientific python stack (Jones et al. 2001; Hunter 2007; van der Walt et al. 2011) and the HDF5 file format (The HDF Group 1997). G. Longhi's color scheme suggestions are gratefully acknowledged.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funding AgencyGrant Number
Kavli FoundationUNSPECIFIED
Gordon and Betty Moore Foundation947
Department of Energy (DOE)DE-AC02-07CH11359
Australian Research CouncilFT150100074
Science and Technology Facilities Council (STFC)UNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Fonds de recherche du Québec - Nature et technologies (FRQNT)UNSPECIFIED
Department of Energy (DOE)DE-AC02-06CH11357
Department of Energy (DOE)DE-AC02-05CH11231
Subject Keywords:cosmology: cosmic background radiation – large-scale structure of the universe
Issue or Number:1
Record Number:CaltechAUTHORS:20191014-111719097
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Official Citation:W. L. K. Wu et al 2019 ApJ 884 70
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:99251
Deposited By: Tony Diaz
Deposited On:14 Oct 2019 18:44
Last Modified:16 Nov 2021 17:45

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